MAXI/GSC detection of a large X-ray flare from the active star binary UV Ceti
ATel #4671; H. Negoro (Nihon U.), S. Nakahira (JAXA), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa (JAXA), T. Mihara, M. Sugizaki, M. Serino, K. Morihana, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Nakano (AGU), H. Tsunemi, M. Sasaki (Osaka U.), M. Nakajima, M. Asada (Nihon U.), Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato, T. Kawamuro (Kyoto U.), Y. Tsuboi, M. Higa (Chuo U.), M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome, Y. Ogawa (Miyazaki U.), K. Yamaoka (ISAS) report on behalf of the MAXI team
on 23 Dec 2012; 14:31 UT
Credential Certification: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)
Subjects: X-ray, Binary, Star, Variables
At 00:21 UT of December 23, 2012,
the MAXI/GSC transient alert system triggered on enhanced X-ray emission from
the position consistent with the active dMe star binary UV Ceti.
The 2-10 keV flux averaged over the 56-second triangular transit was
about 169 ±25 mCrab, corresponding to an X-ray luminosity of
about 3.5e30 ergs/s for 2.7 pc distance.
Note that the luminosity is larger than that of an X-ray flare (~2e29 erg/s)
detected with Chandra in 2001 (Audard et al. 2003, ApJ 589, 983) by a factor of more than 10.
Unfortunately, MAXI could not observed the source until about 6 hours later, 6:32 (UT), and
the upper limit of the flux at the scan transit is ~20 mCrab.
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